Compton heated winds and coronae above accretion disks. I Dynamics

Details Compton heated winds and coronae above accretion disks. I Dynamics Compton heated winds and coronae above accretion disks. I Dynamics

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271...70b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 1, 1983, p. 70-88. Research supported by the Science Research Cou

Astronomy and Astrophysics

Astronomy

285

Accretion Disks, Stellar Coronas, Stellar Mass Accretion, Stellar Winds, X Ray Astronomy, Active Galactic Nuclei, Binary Stars, Hydrodynamic Equations, Quasars, Stellar Mass Ejection, X Ray Binaries, X Ray Sources

Scientific paper

X rays emitted in the inner part of an accretion disk system can heat the surface of the disk farther out, producing a corona and possibly driving off a strong wind. The dynamics of Compton-heated coronae and winds are analyzed using an approximate two-dimensional technique to estimate the mass loss rate as a function of distance from the source of X rays. The findings have important dynamical implications for accretion disks in quasars, active galactic nuclei, X ray binaries, and cataclysmic variables. These include: mass loss from the disk possibly comparable with or exceeding the net accretion rate onto the central compact object, which may lead to unstable accretion; sufficient angular momentum loss in some cases to truncate the disk in a semidetached binary at a smaller radius than that predicted by tidal truncation theories; and combined static plus ram pressure in the wind adequate to confine line-emitting clouds in quasars and Seyfert galaxies.

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